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We study the evolution of supernova core from the beginning of gravitationalcollapse of a 15Msolar star up to 1 second after core bounce. We presentresults of spherically symmetric simulations of core-collapse supernovae bysolving general relativistic neutrino-radiation-hydrodynamics in the implicittime-differencing. We aim to explore the evolution of shock wave in a long termand investigate the formation of protoneutron star together with supernovaneutrino signatures. These studies are done to examine the influence ofequation of state (EOS) on the postbounce evolution of shock wave in the latephase and the resulting thermal evolution of protoneutron star. We make acomparison of two sets of EOS, that is, by Lattimer and Swesty (LS-EOS) and byShen et al.(SH-EOS). We found that, for both EOSs, the core does not explodeand the shock wave stalls similarly in the first 100 milliseconds after bounce.The revival of shock wave does not occur even after a long period in eithercases. However, the recession of shock wave appears different beyond 200milliseconds after bounce, having different thermal evolution of central core.A more compact protoneutron star is found for LS-EOS than SH-EOS with adifference in the central density by a factor of ~2 and a difference of ~10 MeVin the peak temperature. Resulting spectra of supernova neutrinos are differentto the extent that may be detectable by terrestrial neutrino detectors.Comment: 28 pages, 17 figures, accepted by Astrophysical Journa

Postbounce Evolution of Core‐Collapse Supernovae: Long‐Term Effects of the Equation of State